Table 4.

Parameters of the WR features in the optical spectrum of the CSPN of NGC 6905.

IDNatureIonλ0χλcFFWHMEWSNRFλ/FRBEWλ/EWRB
(Å)(eV)(Å)(10−14 erg cm−2 s−1)(Å)(Å)(FRB = 100)(FRB = 100)
(1)(2)(3)(4)(5)(6)(7)(8)(9)(10)(11)(12)
VB
1WRO vi3811138.13811.0206.99 ± 0.4624.8245.9 ± 1.343.6572.74 ± 2.29279.37 ± 0.15
2WRO vi3834138.13834.090.25 ± 0.3623.9102.7 ± 0.643.6249.72 ± 1.30116.69 ± 0.19
BB
3WRC iv465864.54658.053.95 ± 0.5927.877.1 ± 1.120.2149.28 ± 1.7187.55 ± 0.86
4WRHe ii468624.64686.061.52 ± 0.5825.490.4 ± 1.220.2170.23 ± 1.70102.71 ± 0.94
5NebHe ii468624.64686.18.62 ± 0.245.412.7 ± 0.420.223.85 ± 0.6714.39 ± 0.45
6Neb[Ar iv]47114711.01.05 ± 0.195.41.6 ± 0.320.22.91 ± 0.531.80 ± 0.32
RB
7WRC iv580664.55802.836.14 ± 0.1237.488.0 ± 0.465.5100.00 ± 0.47100.00 ± 0.03
other lines
8WRC iv368964.53689.05.06 ± 0.2014.45.7 ± 0.243.614.00 ± 0.566.50 ± 0.22
9WRC iv393364.53932.43.19 ± 0.1918.14.2 ± 0.243.68.83 ± 0.534.73 ± 0.25
10WRHe ii420024.64200.61.29 ± 0.1717.41.8 ± 0.243.63.57 ± 0.472.04 ± 0.25
11WRC iv422764.54226.72.96 ± 0.1818.94.2 ± 0.243.68.19 ± 0.504.72 ± 0.26
12WRC iv444064.54442.81.95 ± 0.2811.02.9 ± 0.420.25.40 ± 0.773.30 ± 0.45
13WRO vi4500138.14498.15.48 ± 0.278.98.2 ± 0.420.215.16 ± 0.759.34 ± 0.43
14WRHe ii454124.64541.05.19 ± 0.4529.97.8 ± 0.720.214.36 ± 1.258.89 ± 0.73
15WRC iv478964.54789.21.99 ± 0.3321.43.4 ± 0.620.25.51 ± 0.913.84 ± 0.62
16WRO v4933113.94933.14.87 ± 0.3830.38.7 ± 0.720.213.48 ± 1.059.92 ± 0.74
17WRO v5100113.95100.03.60 ± 0.4141.56.9 ± 0.820.29.96 ± 1.147.84 ± 0.86
18WRO vi5166138.15166.50.52 ± 0.0611.41.0 ± 0.120.21.44 ± 0.171.15 ± 0.13
19WRO vi5290138.15288.913.13 ± 0.0917.326.4 ± 0.266.836.33 ± 0.2829.94 ± 0.09
20WRHe ii541224.65411.88.49 ± 0.0923.617.9 ± 0.266.823.49 ± 0.2620.34 ± 0.13
21WRC iv547064.55468.66.89 ± 0.1026.6114.9 ± 0.266.819.07 ± 0.2616.91 ± 0.15
22WRO v5600113.95595.02.59 ± 0.0735.55.9 ± 0.265.57.17 ± 0.286.72 ± 0.22
23WRO vi6200138.16198.53.35 ± 0.0819.010.2 ± 0.343.39.27 ± 0.2211.61 ± 0.24
24WRHe ii640624.66406.00.63 ± 0.0311.82.2 ± 0.243.31.74 ± 0.142.51 ± 0.20
25WRHe ii656024.66557.710.95 ± 0.0744.536.7 ± 0.443.330.30 ± 0.3541.69 ± 0.29
26WRO v6740113.96746.31.33 ± 0.1047.95.3 ± 0.443.33.68 ± 0.266.01 ± 0.40
27WRC iv706064.57059.98.54 ± 0.0435.439.0 ± 0.357.923.63 ± 0.1844.31 ± 0.15
Special lines|$^{\dagger }\, ^{\dagger }$|
28stellar emissionNe vii4555207.34552.51.14 ± 0.3014.41.7 ± 0.520.23.15 ± 0.831.96 ± 0.51
29stellar emissionNe vii5666207.35665.41.63 ± 0.0720.43.8 ± 0.265.54.51 ± 0.194.36 ± 0.17
30stellar emissionNe viii6068239.16065.91.51 ± 0.0712.14.2 ± 0.243.34.18 ± 0.194.82 ± 0.21
IDNatureIonλ0χλcFFWHMEWSNRFλ/FRBEWλ/EWRB
(Å)(eV)(Å)(10−14 erg cm−2 s−1)(Å)(Å)(FRB = 100)(FRB = 100)
(1)(2)(3)(4)(5)(6)(7)(8)(9)(10)(11)(12)
VB
1WRO vi3811138.13811.0206.99 ± 0.4624.8245.9 ± 1.343.6572.74 ± 2.29279.37 ± 0.15
2WRO vi3834138.13834.090.25 ± 0.3623.9102.7 ± 0.643.6249.72 ± 1.30116.69 ± 0.19
BB
3WRC iv465864.54658.053.95 ± 0.5927.877.1 ± 1.120.2149.28 ± 1.7187.55 ± 0.86
4WRHe ii468624.64686.061.52 ± 0.5825.490.4 ± 1.220.2170.23 ± 1.70102.71 ± 0.94
5NebHe ii468624.64686.18.62 ± 0.245.412.7 ± 0.420.223.85 ± 0.6714.39 ± 0.45
6Neb[Ar iv]47114711.01.05 ± 0.195.41.6 ± 0.320.22.91 ± 0.531.80 ± 0.32
RB
7WRC iv580664.55802.836.14 ± 0.1237.488.0 ± 0.465.5100.00 ± 0.47100.00 ± 0.03
other lines
8WRC iv368964.53689.05.06 ± 0.2014.45.7 ± 0.243.614.00 ± 0.566.50 ± 0.22
9WRC iv393364.53932.43.19 ± 0.1918.14.2 ± 0.243.68.83 ± 0.534.73 ± 0.25
10WRHe ii420024.64200.61.29 ± 0.1717.41.8 ± 0.243.63.57 ± 0.472.04 ± 0.25
11WRC iv422764.54226.72.96 ± 0.1818.94.2 ± 0.243.68.19 ± 0.504.72 ± 0.26
12WRC iv444064.54442.81.95 ± 0.2811.02.9 ± 0.420.25.40 ± 0.773.30 ± 0.45
13WRO vi4500138.14498.15.48 ± 0.278.98.2 ± 0.420.215.16 ± 0.759.34 ± 0.43
14WRHe ii454124.64541.05.19 ± 0.4529.97.8 ± 0.720.214.36 ± 1.258.89 ± 0.73
15WRC iv478964.54789.21.99 ± 0.3321.43.4 ± 0.620.25.51 ± 0.913.84 ± 0.62
16WRO v4933113.94933.14.87 ± 0.3830.38.7 ± 0.720.213.48 ± 1.059.92 ± 0.74
17WRO v5100113.95100.03.60 ± 0.4141.56.9 ± 0.820.29.96 ± 1.147.84 ± 0.86
18WRO vi5166138.15166.50.52 ± 0.0611.41.0 ± 0.120.21.44 ± 0.171.15 ± 0.13
19WRO vi5290138.15288.913.13 ± 0.0917.326.4 ± 0.266.836.33 ± 0.2829.94 ± 0.09
20WRHe ii541224.65411.88.49 ± 0.0923.617.9 ± 0.266.823.49 ± 0.2620.34 ± 0.13
21WRC iv547064.55468.66.89 ± 0.1026.6114.9 ± 0.266.819.07 ± 0.2616.91 ± 0.15
22WRO v5600113.95595.02.59 ± 0.0735.55.9 ± 0.265.57.17 ± 0.286.72 ± 0.22
23WRO vi6200138.16198.53.35 ± 0.0819.010.2 ± 0.343.39.27 ± 0.2211.61 ± 0.24
24WRHe ii640624.66406.00.63 ± 0.0311.82.2 ± 0.243.31.74 ± 0.142.51 ± 0.20
25WRHe ii656024.66557.710.95 ± 0.0744.536.7 ± 0.443.330.30 ± 0.3541.69 ± 0.29
26WRO v6740113.96746.31.33 ± 0.1047.95.3 ± 0.443.33.68 ± 0.266.01 ± 0.40
27WRC iv706064.57059.98.54 ± 0.0435.439.0 ± 0.357.923.63 ± 0.1844.31 ± 0.15
Special lines|$^{\dagger }\, ^{\dagger }$|
28stellar emissionNe vii4555207.34552.51.14 ± 0.3014.41.7 ± 0.520.23.15 ± 0.831.96 ± 0.51
29stellar emissionNe vii5666207.35665.41.63 ± 0.0720.43.8 ± 0.265.54.51 ± 0.194.36 ± 0.17
30stellar emissionNe viii6068239.16065.91.51 ± 0.0712.14.2 ± 0.243.34.18 ± 0.194.82 ± 0.21

(1) Identification number; (2) nature of the contributing emission line: WR (broad/stellar) or nebular (narrow); (3) ion; (4) rest wavelength in Å; (5) Ionization potential [eV]; (6) observed centre of the line; (7) flux [10−14 erg cm−2 s−1]; (8) full width at half-maximum (FWHM) [Å]; (9) equivalent width (EW) [Å]; (10) continuum signal-to-noise ratio (SNR) closest to the feature; (11) line fluxes normalized to that of the RB. The ratio has been computed adopting F(RB) = 100. (12) EW normalized to that of the RB, adopting EW(RB) = 100. Special lines |$^{\dagger }\, ^{\dagger }$| correspond to high ionization Ne lines from stellar emission origin (Werner, Rauch & Kruk 2007). Only the statistical errors, determined with equations (1) and (2), are shown in this table.

Table 4.

Parameters of the WR features in the optical spectrum of the CSPN of NGC 6905.

IDNatureIonλ0χλcFFWHMEWSNRFλ/FRBEWλ/EWRB
(Å)(eV)(Å)(10−14 erg cm−2 s−1)(Å)(Å)(FRB = 100)(FRB = 100)
(1)(2)(3)(4)(5)(6)(7)(8)(9)(10)(11)(12)
VB
1WRO vi3811138.13811.0206.99 ± 0.4624.8245.9 ± 1.343.6572.74 ± 2.29279.37 ± 0.15
2WRO vi3834138.13834.090.25 ± 0.3623.9102.7 ± 0.643.6249.72 ± 1.30116.69 ± 0.19
BB
3WRC iv465864.54658.053.95 ± 0.5927.877.1 ± 1.120.2149.28 ± 1.7187.55 ± 0.86
4WRHe ii468624.64686.061.52 ± 0.5825.490.4 ± 1.220.2170.23 ± 1.70102.71 ± 0.94
5NebHe ii468624.64686.18.62 ± 0.245.412.7 ± 0.420.223.85 ± 0.6714.39 ± 0.45
6Neb[Ar iv]47114711.01.05 ± 0.195.41.6 ± 0.320.22.91 ± 0.531.80 ± 0.32
RB
7WRC iv580664.55802.836.14 ± 0.1237.488.0 ± 0.465.5100.00 ± 0.47100.00 ± 0.03
other lines
8WRC iv368964.53689.05.06 ± 0.2014.45.7 ± 0.243.614.00 ± 0.566.50 ± 0.22
9WRC iv393364.53932.43.19 ± 0.1918.14.2 ± 0.243.68.83 ± 0.534.73 ± 0.25
10WRHe ii420024.64200.61.29 ± 0.1717.41.8 ± 0.243.63.57 ± 0.472.04 ± 0.25
11WRC iv422764.54226.72.96 ± 0.1818.94.2 ± 0.243.68.19 ± 0.504.72 ± 0.26
12WRC iv444064.54442.81.95 ± 0.2811.02.9 ± 0.420.25.40 ± 0.773.30 ± 0.45
13WRO vi4500138.14498.15.48 ± 0.278.98.2 ± 0.420.215.16 ± 0.759.34 ± 0.43
14WRHe ii454124.64541.05.19 ± 0.4529.97.8 ± 0.720.214.36 ± 1.258.89 ± 0.73
15WRC iv478964.54789.21.99 ± 0.3321.43.4 ± 0.620.25.51 ± 0.913.84 ± 0.62
16WRO v4933113.94933.14.87 ± 0.3830.38.7 ± 0.720.213.48 ± 1.059.92 ± 0.74
17WRO v5100113.95100.03.60 ± 0.4141.56.9 ± 0.820.29.96 ± 1.147.84 ± 0.86
18WRO vi5166138.15166.50.52 ± 0.0611.41.0 ± 0.120.21.44 ± 0.171.15 ± 0.13
19WRO vi5290138.15288.913.13 ± 0.0917.326.4 ± 0.266.836.33 ± 0.2829.94 ± 0.09
20WRHe ii541224.65411.88.49 ± 0.0923.617.9 ± 0.266.823.49 ± 0.2620.34 ± 0.13
21WRC iv547064.55468.66.89 ± 0.1026.6114.9 ± 0.266.819.07 ± 0.2616.91 ± 0.15
22WRO v5600113.95595.02.59 ± 0.0735.55.9 ± 0.265.57.17 ± 0.286.72 ± 0.22
23WRO vi6200138.16198.53.35 ± 0.0819.010.2 ± 0.343.39.27 ± 0.2211.61 ± 0.24
24WRHe ii640624.66406.00.63 ± 0.0311.82.2 ± 0.243.31.74 ± 0.142.51 ± 0.20
25WRHe ii656024.66557.710.95 ± 0.0744.536.7 ± 0.443.330.30 ± 0.3541.69 ± 0.29
26WRO v6740113.96746.31.33 ± 0.1047.95.3 ± 0.443.33.68 ± 0.266.01 ± 0.40
27WRC iv706064.57059.98.54 ± 0.0435.439.0 ± 0.357.923.63 ± 0.1844.31 ± 0.15
Special lines|$^{\dagger }\, ^{\dagger }$|
28stellar emissionNe vii4555207.34552.51.14 ± 0.3014.41.7 ± 0.520.23.15 ± 0.831.96 ± 0.51
29stellar emissionNe vii5666207.35665.41.63 ± 0.0720.43.8 ± 0.265.54.51 ± 0.194.36 ± 0.17
30stellar emissionNe viii6068239.16065.91.51 ± 0.0712.14.2 ± 0.243.34.18 ± 0.194.82 ± 0.21
IDNatureIonλ0χλcFFWHMEWSNRFλ/FRBEWλ/EWRB
(Å)(eV)(Å)(10−14 erg cm−2 s−1)(Å)(Å)(FRB = 100)(FRB = 100)
(1)(2)(3)(4)(5)(6)(7)(8)(9)(10)(11)(12)
VB
1WRO vi3811138.13811.0206.99 ± 0.4624.8245.9 ± 1.343.6572.74 ± 2.29279.37 ± 0.15
2WRO vi3834138.13834.090.25 ± 0.3623.9102.7 ± 0.643.6249.72 ± 1.30116.69 ± 0.19
BB
3WRC iv465864.54658.053.95 ± 0.5927.877.1 ± 1.120.2149.28 ± 1.7187.55 ± 0.86
4WRHe ii468624.64686.061.52 ± 0.5825.490.4 ± 1.220.2170.23 ± 1.70102.71 ± 0.94
5NebHe ii468624.64686.18.62 ± 0.245.412.7 ± 0.420.223.85 ± 0.6714.39 ± 0.45
6Neb[Ar iv]47114711.01.05 ± 0.195.41.6 ± 0.320.22.91 ± 0.531.80 ± 0.32
RB
7WRC iv580664.55802.836.14 ± 0.1237.488.0 ± 0.465.5100.00 ± 0.47100.00 ± 0.03
other lines
8WRC iv368964.53689.05.06 ± 0.2014.45.7 ± 0.243.614.00 ± 0.566.50 ± 0.22
9WRC iv393364.53932.43.19 ± 0.1918.14.2 ± 0.243.68.83 ± 0.534.73 ± 0.25
10WRHe ii420024.64200.61.29 ± 0.1717.41.8 ± 0.243.63.57 ± 0.472.04 ± 0.25
11WRC iv422764.54226.72.96 ± 0.1818.94.2 ± 0.243.68.19 ± 0.504.72 ± 0.26
12WRC iv444064.54442.81.95 ± 0.2811.02.9 ± 0.420.25.40 ± 0.773.30 ± 0.45
13WRO vi4500138.14498.15.48 ± 0.278.98.2 ± 0.420.215.16 ± 0.759.34 ± 0.43
14WRHe ii454124.64541.05.19 ± 0.4529.97.8 ± 0.720.214.36 ± 1.258.89 ± 0.73
15WRC iv478964.54789.21.99 ± 0.3321.43.4 ± 0.620.25.51 ± 0.913.84 ± 0.62
16WRO v4933113.94933.14.87 ± 0.3830.38.7 ± 0.720.213.48 ± 1.059.92 ± 0.74
17WRO v5100113.95100.03.60 ± 0.4141.56.9 ± 0.820.29.96 ± 1.147.84 ± 0.86
18WRO vi5166138.15166.50.52 ± 0.0611.41.0 ± 0.120.21.44 ± 0.171.15 ± 0.13
19WRO vi5290138.15288.913.13 ± 0.0917.326.4 ± 0.266.836.33 ± 0.2829.94 ± 0.09
20WRHe ii541224.65411.88.49 ± 0.0923.617.9 ± 0.266.823.49 ± 0.2620.34 ± 0.13
21WRC iv547064.55468.66.89 ± 0.1026.6114.9 ± 0.266.819.07 ± 0.2616.91 ± 0.15
22WRO v5600113.95595.02.59 ± 0.0735.55.9 ± 0.265.57.17 ± 0.286.72 ± 0.22
23WRO vi6200138.16198.53.35 ± 0.0819.010.2 ± 0.343.39.27 ± 0.2211.61 ± 0.24
24WRHe ii640624.66406.00.63 ± 0.0311.82.2 ± 0.243.31.74 ± 0.142.51 ± 0.20
25WRHe ii656024.66557.710.95 ± 0.0744.536.7 ± 0.443.330.30 ± 0.3541.69 ± 0.29
26WRO v6740113.96746.31.33 ± 0.1047.95.3 ± 0.443.33.68 ± 0.266.01 ± 0.40
27WRC iv706064.57059.98.54 ± 0.0435.439.0 ± 0.357.923.63 ± 0.1844.31 ± 0.15
Special lines|$^{\dagger }\, ^{\dagger }$|
28stellar emissionNe vii4555207.34552.51.14 ± 0.3014.41.7 ± 0.520.23.15 ± 0.831.96 ± 0.51
29stellar emissionNe vii5666207.35665.41.63 ± 0.0720.43.8 ± 0.265.54.51 ± 0.194.36 ± 0.17
30stellar emissionNe viii6068239.16065.91.51 ± 0.0712.14.2 ± 0.243.34.18 ± 0.194.82 ± 0.21

(1) Identification number; (2) nature of the contributing emission line: WR (broad/stellar) or nebular (narrow); (3) ion; (4) rest wavelength in Å; (5) Ionization potential [eV]; (6) observed centre of the line; (7) flux [10−14 erg cm−2 s−1]; (8) full width at half-maximum (FWHM) [Å]; (9) equivalent width (EW) [Å]; (10) continuum signal-to-noise ratio (SNR) closest to the feature; (11) line fluxes normalized to that of the RB. The ratio has been computed adopting F(RB) = 100. (12) EW normalized to that of the RB, adopting EW(RB) = 100. Special lines |$^{\dagger }\, ^{\dagger }$| correspond to high ionization Ne lines from stellar emission origin (Werner, Rauch & Kruk 2007). Only the statistical errors, determined with equations (1) and (2), are shown in this table.

Close
This Feature Is Available To Subscribers Only

Sign In or Create an Account

Close

This PDF is available to Subscribers Only

View Article Abstract & Purchase Options

For full access to this pdf, sign in to an existing account, or purchase an annual subscription.

Close